In 2015, the first direct detection of gravitational waves was reported. Data analysis indicated that the waves had originated from the violent collision of two black holes, which scattered them through space–time as Einstein predicted. That detection was made possible by many advances in measurement technology, mainly vibration isolation of the detector optics, since, at 10 Hz, the motion of the laser‐interferometric detector mirrors is at least one billion times smaller than the seismic motion of the ground. As well, it is difficult to lock the laser in the detection configuration in a large band of the spectrum; this was made possible by using many feedback and feed‐forward control loops. However, in order to meet the many demanding requirements, more than a hundred of such active systems are included in a detector to allow locked acquisition and locked stability to, eventually, reach the desired sensitivity. In this work, challenges faced to reach some of these requirements will be described and we analyze how this scenario impacts the calibration of such detectors. In order to help reduce false alarm rates and provide data for veto systems, in this work we propose a specific kind of resonant‐mass detector to operate in coincidence with laser‐interferometric ones.

中文翻译：

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校准激光干涉重力波探测器的挑战

2015年，首次报道了重力波的直接探测。数据分析表明，波源于两个黑洞的剧烈碰撞，正如爱因斯坦所预言的那样，它们在时空上分散开来。测量技术的许多进步使检测成为可能，主要是探测器光学系统的隔振，因为在10 Hz时，激光干涉探测器镜的运动至少比地面的地震运动小十亿倍。同样，很难将激光器锁定在大光谱波段的检测配置中。通过使用许多反馈和前馈控制回路，这才成为可能。但是，为了满足许多苛刻的要求，检测器中包含一百多个这样的有源系统，以允许锁定的采集和锁定的稳定性，最终达到所需的灵敏度。在这项工作中，将描述达到某些要求所面临的挑战，我们将分析这种情况如何影响此类检测器的校准。为了帮助减少误报率并为否决系统提供数据，在这项工作中，我们提出了一种特殊的共振质量检测器，使其与激光干涉检测器同时工作。